Longer-period planets have comparatively long tidal alignment timescales, especially around hot stars. The small spin-orbit angles observed for exoplanets around hot stars, therefore, may suggest that protoplanetary disks tend to be aligned at the time of gas dispersal [1]}, [2]}. In this case, hot Jupiters would need to obtain their misalignments after the protoplanetary disk has dispersed, favoring high-eccentricity migration as an important formation mechanism [3]}, [4]}. Most of the misaligned planets at \(P>5\)  days are on eccentric orbits, suggesting that interactions with stellar or planetary companions in the systems may have induced both elevated obliquities and eccentricities.
